Symmetries in String Theory

1. Symmetries in String Theory Michael Dine University of California, Santa Cruz DeWolfe, Giryavets, Kachru and Taylor Z. Sun and M. D. G. Festuccia, A. Morisse, K. van den Broek, M.D.

2. I have learned a lot from Andrei through the years, starting long before I met him. As a very green postdoc, his papers introduced me to finite temperature field theory (the one below I well remember reading in my future spouse’s apartment in San Antonio), issues in tunneling, phase transitions in the early universe… All of these had a profound impact on my own research and thinking. Meeting Andrei, and working with him, was an even greater pleasure.

3. Symmetries in Particle Physics During the last three decades, it has been dogma that symmetries are a good thing in particle physics, and they have played a central role in conjectures about physics beyond the Standard Model. Gauge symmetries, discrete symmetries, supersymmetry natural, plausible. Explanations of hierarchy, fermion masses, other possible features of physics beyond the Standard Model. As we await the LHC, this dogma merits closer scrutiny. Professor of dogma and of the history of dogmas at the University of Regensburg

4. Indeed, the lesson learned by many of those who experienced the Old Soviet Union is that one should be skeptical of dogma. That could be called the theory of symmetry: all governments and regimes to a first approximation are bad, all peoples are oppressed, and all are threatened by common dangers.”  (A. Sakharov)  I will be politically neutral today. Due to recent developments in string theory, symmetry is in danger of being dethroned (purged), but the situation, I claim, is as yet unsettled.

5. In string theory, questions of symmetry are often sharp. We know that in critical string theories: • There are no global continuous symmetries in string theory, as expected in a theory of gravity (Banks, Dixon). • Gauge symmetries arise by several mechanisms. • N=1 supersymmetry, warping, technicolor, as conjectured to solve the hierarchy problem, all arise in string theory. • Discrete symmetries arise in string theory. Generally can be thought of as discrete gauge symmetries.

6. But until recently, we had little idea how string theory might be related to the universe about us, so it was not clear what to make of these observations. In what sense are any of these features generic?

7. The Landscape provides a framework in which these questions can be addressed. There is much about the landscape which is controversial. The very existence of such a vast set of metastable states can hardly be viewed as reliably established; the mechanisms for transitions between states, and by which states might be selected are not understood in anything resembling a reliable or systematic scheme. But for the first time, we have a model in which to address a variety of questions. I claim that the easiest questions to study are precisely those associated with naturalness and symmetries. These can be addressed in model landscapes. Today, mainly IIB flux landscape.

8. An “easy” question: How common are discrete symmetries? We will argue that they are expensive; only a tiny fraction of states exhibit discrete R symmetries (Z2 may be common). Harder: it is known (KKLT, Douglas et al) that approximate N=1 susy, warping, pseudomoduli are common features in the landscape. But just how common? Can we just count (already hard)? Cosmology important?

9. Discrete Symmetries While continuous symmetries don’t arise in critical string theory, discrete symmetries often arise. Many can be thought of as unbroken subgroups of rotations in compactified dimensions; as such, R symmetries. E.g. Z3 orbifold: 60o Invariant under zi e2 p i/6 zi, for each i Many Calabi-Yau vacua exhibit intricate discrete symmetries at points in their moduli spaces.

10. Symmetries in Flux Vacua Fluxes and fields transform under symmetries. If we are to preserve a symmetry, it is important that we turn on no fluxes that break the symmetry, and that that vev’s of fields preserve the symmetry. One can survey, e.g., IIB orientifold theories compactified on Calabi-Yau (KKLT type models).

11. Result: Discrete Symmetries are Rare Why a large number of states in landscape: Nb possible choices of flux(N a typical flux; b the number of fluxes, both large, say N =10, b=300) In CY spaces, one finds typically at most 1/3 of fluxes invariant, b reduced by 1/3, and Simply counting might be too naïve; we’ll return to this question.

12. Possible Explanations for Hierarchy in the Landscape • SUSY states: exponentially large numbers; within these, hierarchies in a finite fraction of states – conventional naturalness. • Warping (with or without susy): likely occurs in a finite fraction of states (Douglas et al). So another possible explanation of hierarchies, dual to technicolor. • Simply very, very many states; a tiny fraction – but a large number -- exhibit hierarchies. In all cases, anthropic considerations might be relevant.

13. Branches of the Landscape Three distinct branches identified in IIB: • Non-supersymmetric • Supersymmetric with logarithmic distribution of susy breaking scales P(m3/2) = dm3/2/m3/2 • Supersymmetry with approximate R symmetries: P(m3/2) = dm3/2/m3/23

14. Perhaps no “rational” (=symmetry) Explanation of Hierarchy Non-susy states might vastly outnumber susy [or warped, technicolored] states (Douglas; Silverstein). So there might be many, many more states with light Higgs without susy than with. (E.g. anthropic selection for light Higgs?). Perhaps few or no TeV signals; light Higgs most economical. (Even “split susy” an optimistic outcome.)

15. Counting of states, statistics, interesting, but probably naïve to think this is the only consideration (though success of Weinberg argument suggests some level of democracy among states). Surely, though, it is important to think about cosmology.

16. A Primitive Cosmological Question: Metastability A candidate “state” (=stationary point of some effective action), say with small L, is surrounded by an exponentially large number of states with negative L. (Possibly also many states with positive L) Metastability only if decay rate to every one of these states is small. One more anthropic accident? Or insured by some general principle? A ``selection principle”? (or more precisely, a pointer to the types of states which might actually exist?)

17. Asymptotic weak coupling region Small positive L AdS

18. Stability in the Landscape Naïve landscape picture: large number of possible fluxes (b) taking many different values (Ni, i=1,…, b; N » 10, say, b » 100). Structure of potential (IIB, semiclassical, large volume): V(z) = Ni Nj fij(zI) Focus on states with small L. Many nearby states with negative L

19. Typical Decay Rates (non-susy) These naïve scalings of tensions and cosmological constants can be checked in explicit string constructions, e.g. GKP.

20. Not really a surprise. In general, without small parameters, expect tunneling very rapid. Bousso-Polchinski model gives similar scalings; BP assumed, that in every state, there was a small parameter which accounts for metastability. Crucial to much thinking about eternal inflation. Critical for the candidate small cc states which could describe our universe. In a landscape, this is a strong assumption. For typical choice of fluxes, no small parameter. But since there are many nearby states, it is critically important that all tunneling amplitudes be small. E.g. if D N < 4 then 3b decay channels, all of which must be suppressed (3100¼ 1048).

21. Seek classes of states which are metastable. • Weak (string) coupling by itself not sufficient. • From our formulas above, we see large volume stable. Not clearly from any existing analysis why a typical (dS) state should have large volume; may single out an important subset. • No evidence that warping enhances stability • Supersymmetry? Actually, this is the easy (and well-known) one.

22. With zero c.c., can define global energy, momentum, and supersymmetry charges. Obey: {Qa,Qb} = Pm (gm)ab As a consequence, all field configurations have positive energy, so exact supersymmetry in flat space should be stable (note this is true even if potential is negative in some regions of field space). [Thanks to T. Banks,E. Witten and others] Expect that if nearly supersymmetric, nearly flat, decay amplitudes are zero or exponentially small (exp (-M4/F2)). Can check in many simple examples.

23. A Path To A Symmetric Universe • Non-susy, metastable states: perhaps not particularly numerous compared to susy states. Then hierarchy (even with anthropic considerations) might favor “low energy supersymmetry” • KKLT vacua: surrounded by numerous susy, non-susy AdS states. Cosmological evolution into such states might be problematic. • Symmetric states (R symmetric states) might be cosmological attractors within a picture of eternal inflation.

24. V Perhaps R Symmetry points cosmological attractors? Don’t give up on the symmetric points yet!

25. R Symmetric states as attractors? R symmetry: vanishing W (classically). Obtain by setting many fluxes to zero. Nearby states: turn on “small” fluxes. Types of flux: NI (symmetric); na (break symmetry), NIÀ na Following Kachru et al, Douglas et al, treat fluxes, and the labels a as continuous. Vacuum energy: V= s dw |n(w)|2 a(w) a(w) will typically have different signs over different ranges of w; correspondingly n+, n-.

26. Decays will disfavor the symmetric vacuum; n+(w) will tend to decrease, but n-(w) will grow. There may, however, be branches with a(w)>0 for all w. Then typical decay chains will lead to the symmetric vacuum. These issues are currently under investigation.

27. Status of the Old Dogma Perhaps we are seeing the beginnings of a picture for how predictions (low energy susy? large compactification volume? Perhaps a pattern of discrete symmetries?) might emerge from string theory. As another expatriate friend of mine used to say, not everything that we were told growing up was wrong.

32. Aside on Small Volume It is tempting not to think about small volume, since few tools, in general. But KKLT analysis illustrates how small volume may arise. Standard story: small W0, large r. Argue distribution of W0 is uniform at small W0. But if W0 large, expect susy minima at small r, with a uniform distribution of <W>. So expect that, while can’t calculate, many states with large AdS radius, small compactification volume (Kachru).

33. Large Compactification Volume, Weak Coupling These results confirm our earlier estimates. Large volume does lead to suppression of decay amplitudes. Sb» V2/N3 Even for weak coupling, however, there are decay channels with no suppression by powers of t. So to obtain large number of stable, large volume states, need V » N3/2. In IIB case, little control over volume (except KKLT: approximate susy, large volume). Can model this with IIA theories (but AdS), Silverstein’s constructions. These suggest that there might be many metastable large volume, dS states.

34. Warping No evidence that warping enhances stability. We did not see any growth of tensions with z-1 in GKP analysis. More generally, if a collapsing cycle, as in Giddings, Kachru, Polchinski, then can change fluxes on cycles which are “far away” with little effect on the warping; earlier estimates seem to apply.

35. Quintic in CP4

36. Branches of the landscape (Terminology refers to classical analysis; real distinction is in statistics).

37. Supersymmetry in the IIB Landscape • IIB landscape as a model; suspect some observations below generic. • Possesses an exponentially large set of flux states with N=1 supersymmetry (KKLT, Douglas et al). • A large, possibly infinite set of non-supersymmetric states. Douglas, Denef count by introducing a cutoff on the scale of susy breaking (more on rationale later). Most states near cutoff.

38. Remark: Tempting to believe that non-susy states, I.e. non-susy stationary points of some effective action, are more typical than susy, which seems special. On more thought, might be true, but not obvious. E.g. not true of renormalizable susy models. Not clear if true if IIB on Calabi-Yau. Real non-susy constuctions limited, hard to draw a general conclusion.

39. Known classes of states in the landscape: • N=1 supersymmetric • Weak string coupling • Large volume • Warping • Pseudomoduli • I’ll report some preliminary investigations of the (meta)stability of these classes of states.

40. KKLT V e-r0 r N KKLT KKLT as example, But general Fijk

41. Much of what I will say is tentative. Most work on the landscape has involved supersymmetric or nearly supersymmetric states (also non-susy AdS); features of dS, non-susy states [Douglas, Silverstein] less throughly studied, but it is precisely these states which are at issue. I will also indulge in a conjecture: certain symmetric states might be cosmological attractors. Hard to establish, but I think plausible, and again relatively simple within the space of ideas about string cosmology.